 |
Figure 1: Archival FORS1 image of M 83 with the five cluster fibre positions and three galaxy background fibre positions indicated. |
| Open with DEXTER | |
In the text
 |
Figure 2:
Pipeline-reduced spectrum of the K1 giant HD 159821, normalised and
corrected to rest wavelength, over the wavelength range
 .
The two lines of the Ca II triplet that
are contained in our data (
 )
are marked. The other line of the Ca II
triplet (
 )
lies on the gap between the two CCDs,
which is also indicated. The
major telluric features in this spectral range are also marked. |
| Open with DEXTER | |
In the text
 |
Figure 3:
Best fit of broadening for the K2 III template HD 123833 (blue line)
to our normalised FLAMES+UVES cluster 805 spectrum (black line)
for the `Both CaT' case of
 .
The spectral regions included in the fit are shown where the red line
is at 1.5.
Also included in this figure is the standard echelle UVES spectrum of
cluster 805 from Larsen & Richtler (2004) (grey line), offset
at -1.
See the online journal for a colour image. |
| Open with DEXTER | |
In the text
 |
Figure 4:
Plot of velocity dispersion measured from a 
minimisation
between the five template stars and a simple model cluster spectrum
with
in the `No CaT'
case against the signal-to-noise ratio (SNR) of the model cluster.
The mean velocity dispersion measured is also plotted.
The dashed lines represent the uncertainty, as measured by the
standard deviation if the values, on this mean.
The dotted line shows the true velocity dispersion of the model
cluster.
See the online journal for a colour image.
|
| Open with DEXTER | |
In the text